The bolometric quasar luminosity function at z = 0 − 7
2020
In this paper, we provide updated constraints on the bolometric quasar luminosity function (QLF) from 푧 = 0
to 푧 = 7. The constraints are based on an observational compilation that includes observations in the rest-frame
IR, B band, UV, soft and hard X-ray in past decades. Our method follows Hopkins et al. 2007 with an updated
quasar SED model and bolometric and extinction corrections. The new best-fit bolometric quasar luminosity
function behaves qualitatively different from the Hopkins et al. 2007 model at high redshift. Compared with
the old model, the number density normalization decreases towards higher redshift and the bright-end slope
is steeper at 푧 & 2. Due to the paucity of measurements at the faint end, the faint end slope at 푧 & 5 is quite
uncertain. We present two models, one featuring a progressively steeper faint-end slope at higher redshift
and the other featuring a shallow faint-end slope at 푧 & 5. Further multi-band observations of the faint-end
QLF are needed to distinguish between these models. The evolutionary pattern of the bolometric QLF can
be interpreted as an early phase likely dominated by the hierarchical assembly of structures and a late phase
likely dominated by the quenching of galaxies. We explore the implications of this model on the ionizing
photon production by quasars, the CXB spectrum, the SMBH mass density and mass functions. The predicted
hydrogen photoionization rate contributed by quasars is subdominant during the epoch of reionization and
only becomes important at 푧 . 3. The predicted CXB spectrum, cosmic SMBH mass density and SMBH
mass function are generally consistent with existing observations.
- Correction
- Source
- Cite
- Save
- Machine Reading By IdeaReader
0
References
0
Citations
NaN
KQI